Multifrequency studies of the peculiar quasar 4C+21.35 during the 2010 flaring activity

The discovery of rapidly variable Very High Energy ( VHE; E &gt; 100 GeV). - ray emission from 4C + 21.35 ( PKS 1222+ 216) by MAGIC on 2010 June 17, triggered by the high activity detected by the Fermi Large Area Telescope ( LAT) in high energy ( HE; E &gt; 100 MeV). - rays, poses intriguing questions on the location of the. - ray emitting region in this flat spectrum radio quasar. We present multifrequency data of 4C + 21.35 collected from centimeter to VHE during 2010 to investigate the properties of this source and discuss a possible emission model. The first hint of detection at VHE was observed by MAGIC on 2010 May 3, soon after a gamma- ray flare detected by Fermi-LAT that peaked on April 29. The same emission mechanism may therefore be responsible for both the HE and VHE emission during the 2010 flaring episodes. Two optical peaks were detected on 2010 April 20 and June 30, close in time but not simultaneous with the two gamma- ray peaks, while no clear connection was observed between the X-ray and gamma- ray emission. An increasing flux density was observed in radio and mm bands from the beginning of 2009, in accordance with the increasing gamma- ray activity observed by Fermi-LAT, and peaking on 2011 January 27 in the mm regime ( 230 GHz). We model the spectral energy distributions ( SEDs) of 4C + 21.35 for the two periods of the VHE detection and a quiescent state, using a one-zone model with the emission coming from a very compact region outside the broad line region. The three SEDs can be fit with a combination of synchrotron self-Compton and external Compton emission of seed photons from a dust torus, changing only the electron distribution parameters between the epochs. The fit of the optical/UV part of the spectrum for 2010 April 29 seems to favor an inner disk radius of &lt; six gravitational radii, as one would expect from a prograde-rotating Kerr black hole.</p

Multi-messenger observations of a binary neutron star merger

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40+8-8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Mo. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One- Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta

Proposta educacional virtual sobre atendimento da ressuscitação cardiopulmonar no recém-nascido Propuesta educativa virtual para la atención de la reanimación cardiopulmonar en el recién nacido Virtual educational proposal in cardiopulmonary resuscitation for the neonate care

O objetivo deste estudo foi desenvolver uma proposta educacional virtual, utilizando recursos multimídia, visando inovar, dinamizar e diversificar espaços de comunicação e interação, favorecendo o processo de ensino aprendizagem autônomo e reflexivo do enfermeiro. Este trabalho constitui-se de uma pesquisa aplicada, seguindo as fases cíclicas e interativas de concepção e planejamento, desenvolvimento e implementação. A proposta educacional foi desenvolvida na plataforma TelEduc, utilizando ferramentas de organização, de conteúdo, de comunicação, do aluno e do administrador. Os módulos de ensino referiram-se as seguintes temáticas: Módulo 1 - Fundamentos de anatomia e fisiologia cardíacas do recém-nascido; Módulo 2 - Fatores de risco para ocorrência da parada cardiorrespiratória no recém-nascido; Módulo 3 - Planejamento da assistência de enfermagem; Módulo 4 - Medicações empregadas na parada cardiorrespiratória no recém-nascido; e Módulo 5 - Atendimento da parada cardiorrespiratória no recém-nascido. Este projeto pode contribuir com a inovação do ensino em enfermagem a partir de uma proposta educacional virtual sobre um tema de relevância que é o atendimento da ressuscitação cardiopulmonar do recém-nascido.<br>El objetivo de este estudio fue desarrollar una propuesta educativa virtual haciendo uso de recursos multimedia, pretendiendo innovar, dinamizar y diversificar espacios de comunicación e interacción, facilitando el proceso de enseñanza y aprendizaje autónomo y reflexivo del enfermero. Este trabajo se constituye de una investigación aplicada, siguiendo las fases cíclicas e interactivas de concepción y planeamiento, desarrollo e implementación. La propuesta educativa fue desarrollada sobre la plataforma TelEduc, utilizando herramientas de organización, de contenido, de comunicación, del alumno y del administrador. Los módulos de enseñanza se refirieron a las siguientes temáticas: Módulo 1 - Fundamentos de anatomía y fisiología cardiaca del recién nacido; Módulo 2 - Factores de riesgo para la ocurrencia de paro cardiorrespiratorio en el recién nacido; Módulo 3 - Planeamiento de los cuidados de enfermería; Módulo 4 - Medicamentos utilizados en el paro cardiorrespiratorio del recién nacido, y Módulo 5 - Atención del paro cardiorrespiratorio en el recién nacido. Este estudio puede contribuir a la innovación en la enseñanza de la enfermería a partir de una propuesta educativa virtual referida a un tema de alta relevancia como lo es la atención de la resucitación cardiopulmonar del recién nacido.<br>The purpose of this study was to develop an educational proposal using virtual multimedia resources, to innovate, stimulate and diversify areas of communication and interaction, facilitating nurses' autonomous and reflexive process of teaching and learning. This is an applied research, following the cyclical and interactive phases of designing, planning, developing and implementing. The educational proposal was developed on the TelEduc platform, using specific tools for content organization and communication between students and administrator. The teaching modules were on the following themes: Module 1 - Fundamentals of the heart anatomy and physiology in newborns; Module 2 - Risk factors for the occurrence of cardiorespiratory arrest in newborns; Module 3 - Planning nursing care; Module 4 - Medications used in cardiopulmonary arrests in newborns; and Module 5 - Cardiorespiratory arrest care in newborns. This study may contribute to innovating teaching in nursing from a virtual educational proposal on the important issue of newborn cardiopulmonary resuscitation care

Search for cosmic-ray-induced gamma-ray emission in galaxy clusters

Current theories predict relativistic hadronic particle populations in clusters of galaxies in addition to the already observed relativistic leptons. In these scenarios hadronic interactions give rise to neutral pions which decay into γ rays that are potentially observable with the Large Area Telescope (LAT) on board the Fermi space telescope. We present a joint likelihood analysis searching for spatially extended γ-ray emission at the locations of 50 galaxy clusters in four years of Fermi-LAT data under the assumption of the universal cosmic-ray (CR) model proposed by Pinzke &amp; Pfrommer. We find an excess at a significance of 2.7σ, which upon closer inspection, however, is correlated to individual excess emission toward three galaxy clusters: A400, A1367, and A3112. We discuss these cases in detail and conservatively attribute the emission to unmodeled background systems (for example, radio galaxies within the clusters).Through the combined analysis of 50 clusters, we exclude hadronic injection efficiencies in simple hadronic models above 21% and establish limits on the CR to thermal pressure ratio within the virial radius, R 200, to be below 1.25%-1.4% depending on the morphological classification. In addition, we derive new limits on the γ-ray flux from individual clusters in our sample. © 2014. The American Astronomical Society. All rights reserved

FERMI LARGE AREA TELESCOPE THIRD SOURCE CATALOG

We present the third Fermi Large Area Telescope (LAT) source catalog (3FGL) of sources in the 100 MeV-300 GeV range. Based on the first 4 yr of science data from the Fermi Gamma-ray Space Telescope mission, it is the deepest yet in this energy range. Relative to the Second Fermi LAT catalog, the 3FGL catalog incorporates twice as much data, as well as a number of analysis improvements, including improved calibrations at the event reconstruction level, an updated model for Galactic diffuse γ-ray emission, a refined procedure for source detection, and improved methods for associating LAT sources with potential counterparts at other wavelengths. The 3FGL catalog includes 3033 sources above significance, with source location regions, spectral properties, and monthly light curves for each. Of these, 78 are flagged as potentially being due to imperfections in the model for Galactic diffuse emission. Twenty-five sources are modeled explicitly as spatially extended, and overall 238 sources are considered as identified based on angular extent or correlated variability (periodic or otherwise) observed at other wavelengths. For 1010 sources we have not found plausible counterparts at other wavelengths. More than 1100 of the identified or associated sources are active galaxies of the blazar class; several other classes of non-blazar active galaxies are also represented in the 3FGL. Pulsars represent the largest Galactic source class. From source counts of Galactic sources we estimate that the contribution of unresolved sources to the Galactic diffuse emission is ∼3% at 1 GeV

Inferred cosmic-ray spectrum from Fermi large area telescope γ-ray observations of Earth's limb.

Recent accurate measurements of cosmic-ray (CR) species by ATIC-2, CREAM, and PAMELA reveal an unexpected hardening in the proton and He spectra above a few hundred GeV, a gradual softening of the spectra just below a few hundred GeV, and a harder spectrum of He compared to that of protons. These newly discovered features may offer a clue to the origin of high-energy CRs. We use the Fermi Large Area Telescope observations of the γ-ray emission from Earth's limb for an indirect measurement of the local spectrum of CR protons in the energy range ∼90  GeV-6  TeV (derived from a photon energy range 15 GeV-1 TeV). Our analysis shows that single power law and broken power law spectra fit the data equally well and yield a proton spectrum with index 2.68±0.04 and 2.61±0.08 above ∼200  GeV, respectively

The second Fermi large area telescope catalog of gamma-ray pulsars

This catalog summarizes 117 high-confidence ≥0.1 GeV gamma-ray pulsar detections using three years of data acquired by the Large Area Telescope (LAT) on the Fermi satellite. Half are neutron stars discovered using LAT data through periodicity searches in gamma-ray and radio data around LAT unassociated source positions. The 117 pulsars are evenly divided into three groups: millisecond pulsars, young radio-loud pulsars, and young radio-quiet pulsars. We characterize the pulse profiles and energy spectra and derive luminosities when distance information exists. Spectral analysis of the off-peak phase intervals indicates probable pulsar wind nebula emission for four pulsars, and off-peak magnetospheric emission for several young and millisecond pulsars. We compare the gamma-ray properties with those in the radio, optical, and X-ray bands. We provide flux limits for pulsars with no observed gamma-ray emission, highlighting a small number of gamma-faint, radio-loud pulsars. The large, varied gamma-ray pulsar sample constrains emission models. Fermi's selection biases complement those of radio surveys, enhancing comparisons with predicted population distributions. © 2013. The American Astronomical Society. All rights reserved.